Most of the parameters change with the added AGN contribution in comparison to
real values, with gradually larger differences being observed as the
AGN contribution to the total flux increases. In Table REF , the effect of the AGN has been measured using the median values of
each parameter and each sample (total and for different morphological types), measured on original images (param_orig) and after adding different AGN contributions
(param_AGN), such as: (param_AGN - param_orig)/param_orig. A total number of sources with measured parameters under each sample is also listed in the table. CCON is one of the most sensitive parameters to AGN contribution, facing 22% and 46% of
change (toward higher values) in case of 10% and 25% of added AGN contribution, respectively. On the other side, ASYM is one of the parameters that almost doesn't change independently on AGN contribution. As can be seen in Fig. REF  it takes median values between 0 and 0.13, and therefore we are not listing any values for this parameter in Table REF . This parameter has been measured for 72%, 91%, 71%, 61%, and 66% of the total sample, early-type, early-spiral, late-spiral, and peculiar galaxies, respectively. After ASYM, GINI is the least affected parameter
changing only 8%, 16%, 27%, and 37% for 10% 25%,
50%, and 75% of AGN contribution, respectively. Up to 10% of AGN, CABR and M20 show 10-15% of change. Similar to CABR and M20, SMOOTH is also
showing a low level of contamination below 25% of AGN contribution, however, this parameter is very sensitive to
noise, as shown previously [1]}, [2]}, [3]}, and it could be measured properly for a very small
sub-sample (44%) of the total number of galaxies (see Table REF ). In general, we can observe that AGN
contribution to the total flux of 25% and above produce significant changes in the parameters of \(\gtrsim \)  30% (or \(\gtrsim \)  20% in the case of GINI and M20), except in the case of ASYM.
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